• Bulletin of the Korean Mathematical Society
• /
• v.20 no.2
• /
• pp.95-97
• /
• 1983

In this paper, we show a necessary and sufficient condition for QHC spaces to be S-closed. T. Thomson introduced S-closed spaces in [2]. A topological space X is said to be S-closed if every semi-open cover of X admits a finite subfamily such that the closures of whose members cover the space, where a set A is semi-open if and only if there exists an open set U such that U.contnd.A.contnd.Cl U. A topological space X is quasi-H-closed (denote QHC) if every open cover has a finite subfamily whose closures cover the space. If a topological space X is Hausdorff and QHC, then X is H-closed. It is obvious that every S-closed space is QHC but the converse is not true [2]. In [1], Cameron proved that an extremally disconnected QHC space is S-closed. But S-closed spaces are not necessarily extremally disconnected. Therefore we want to find a necessary and sufficient condition for QHC spaces to be S-closed. A topological space X is said to be semi-locally S-closed if each point of X has a S-closed open neighborhood. Of course, a locally S-closed space is semi-locally S-closed.

• The Bulletin of The Korean Astronomical Society
• /
• v.41 no.2
• /
• pp.43.3-43.3
• /
• 2016

We present a library of high-resolution (R~45,000) and high signal-to-noise ratio ($S/N{\geq}200$) near-infrared spectra of 147 standard stars. High quality spectra were obtained with Immersion GRating INfrared Spectrograph (IGRINS) covering the full range of H ($1.496-1.795{\mu}m$) and K ($2.080-2.460{\mu}m$) bands. The targets are mainly selected as MK standard stars which have well-defined spectral types and luminosity classes, and cover a wide range of effective temperatures and surface gravities. The spectra were corrected for telluric absorption lines and absolute flux calibrated using Two Micron All Sky Survey (2MASS) photometry. We find new spectral indices in H and K bands and provide their EWs. We describe empirical relations between the measured EWs and stellar atmosphere parameters such as effective temperature and surface gravity.

• Journal of the Korean Institute of Educational Facilities
• /
• v.8 no.4
• /
• pp.5-15
• /
• 2001

The purpose of this study is to clarify the using condition and requirement for outdoor space between the parallel types of elementary school buildings focused on Chungbuk province in Korea. Consequently, we investigated the actual conditions of students and teachers, using conditions of outdoor space between school buildings. The summary of outdoor space can be given below. 1) In the using condition of outdoor spaces, most of them have path & covered walks, garden, playground and soon. The distances between neighboring building fixed, the use and quality of outdoor space is differently to spatial configuration of school buildings. For example, garden functions as itself in case of D/H>3, but the other space to observe in D/H>3. 2) In the requirements of outdoor spaces, the amount of scatter number of classmates and teachers is wide. The favoring outdoor space is the woods to take a rest by oneself, the demanding outdoor space is almost a resting place like a school store in case of classmates and the natural facilities like ponds garden pagora in teachers.

• Journal of Astronomy and Space Sciences
• /
• v.11 no.2
• /
• pp.208-231
• /
• 1994

We have undertaken CCD observations of fie이 standard stars with H$\beta$ photometric system to investigate the reliability of H$\beta$ CCD photometry. Flat fielding with dome flat and sky flat for H$\beta$w and H$\beta$n filter was compared with that of B filter in UBV system and, from these, we have not found any difference. It was confirmed that there is a good linear relationship between our H$\beta$ values observed with 2.3m reflector and standard values. However, H$\beta$ values observed with 60cm reflector at Sobaeksan Astronomy Observatory showed very poor relationship. To investigate the accuracy of H$\beta$ CCD photometry for fainter objects, open cluster NGC2437 was observed and reduced with DoPHOT, and the results were compared with those for photoelectric photometry of Stetson(1981).

• Journal of applied mathematics & informatics
• /
• v.40 no.5_6
• /
• pp.1129-1135
• /
• 2022

The purpose of this research is to find an extension of the renowned Chernoff theorem on standard operator algebra. Infact, we prove the following result: Let H be a real (or complex) Banach space and 𝓛(H) be the algebra of bounded linear operators on H. Let 𝓐(H) ⊂ 𝓛(H) be a standard operator algebra. Suppose that D : 𝓐(H) → 𝓛(H) is a linear mapping satisfying the relation D(AⁿBⁿ) = D(Aⁿ)Bⁿ + AⁿD(Bⁿ) for all A, B ∈ 𝓐(H). Then D is a linear derivation on 𝓐(H). In particular, D is continuous. We also present the limitations on such identity by an example.

• The Bulletin of The Korean Astronomical Society
• /
• v.36 no.2
• /
• pp.150.2-150.2
• /
• 2011

Volume Phase Holographic (VPH) gratings are getting more popular as dispersion elements in spectrographs. High efficiency, compact configuration, and easy handling are driving many visual spectrographs to use VPH gratings for their main dispersers or for their cross-dispersers in higher resolution spectrographs. More recently, VPH gratings are being adopted in near-infrared by some spectrographs and by a number of next generation instrument projects. IGRINS (Immersion Grating Infrared Spectrograph) uses a VPH grating as a cross-disperser in each H or K band arm. J or H band performance of VPH gratings has been proven by other instruments. But K-band VPH gratings are new to the field. In this presentation, we are going to present test results we have got so far for verification of H-band VPH gratings and development of K-band VPH gratings.

• Journal of Astronomy and Space Sciences
• /
• v.12 no.2
• /
• pp.204-215
• /
• 1995

We observed SL-9 impact sites on Jupiter with a CCD and a R filter on the KyungHee University 30-inch telescope between July 17 and September 3, 1994. We identified impact sites of A, C, E, G, H, K, L, Q1, W and G-group, We calculated the moving velocity relative to System II and rotation period of the G, L sites to be from -8.0 to 8.8m/s, and $9^h55^m39.4^s\pm34^s$, respectively. The diameters of G and L sites in our first observation were $1.95\times10^4km,\;and\;2.20\times10^4km$, respectively. In particular, we investigated the evolution of the impact sites by calculating the diffusing rates of the impact clouds.

• The Bulletin of The Korean Astronomical Society
• /
• v.36 no.1
• /
• pp.83.1-83.1
• /
• 2011

We report multi-epoch, simultaneous 22 GHz water and 44 GHz Class I methanol maser line survey towards 180 intermediate-mass young stellar objects, including 14 Class 0, 19 Class I objects, and 147 Herbig Ae/Be stars. We detected $H_2O$ and $CH_3OH$ maser emission towards 16 (9%) and 10 (6%) sources with one new $H_2O$ and six new $CH_3OH$ maser sources. The detection rates of both masers rapidly decrease as the central (proto)stars evolve, which is contrary to the trends in high-mass star-forming regions. This suggests that the excitations of the two masers are closely related to the evolutionary stage of the central (proto)stars and the circumstellar environments. $H_2O$ maser velocities deviate on average 9 km s-1 from the ambient gas velocities whereas $CH_3OH$ maser velocities well match with. For both maser emissions, large velocity difference (${\mid}v_{H2O}-v_{sys}{\mid}\;>\; 10kms^{-1}\; and\;{\mid}v_{CH3OH}-v_{sys}{\mid}\;>\;1kms^{-1}$) is mostly confined to Class 0 objects. The formation and disappearance of $H_2O$ maser lines are frequent and the integrated intensities of them change up to two orders of magnitude. In contrast, $CH_3OH$ maser lines usually show no significant change in the intensity, shape, and velocity. This consistent with the previous suggestion that $H_2O$ maser emission originates from the base of an outflow while 44 GHz Class I $CH_3OH$ maser emission arises from the interaction region of the outflow with the ambient gas. The isotropic maser luminosities are well correlated with the bolometric luminosities of the central the objects. The fitted relations are $L_{H2O}=1.71{\ast}10^{-9}(L_{bol})^{0.97}$ and $L_{CH3OH}=1.71{\ast}10^{-10}(L_{bol})^{1.22}$.

• The Bulletin of The Korean Astronomical Society
• /
• v.32 no.2
• /
• pp.35.2-35.2
• /
• 2007

• Bulletin of the Korean Space Science Society
• /
• 1999.09a
• /
• pp.65-65
• /
• 1999

No Abstract, See Full Text